1. NEW: hochunk3d_20140131,
the latest version of the HOCHUNK radiative equilibrium code:
fortran-95, 3-D, and more,
all explained in this companion paper (Whitney et
al. 2013, ApJS, 207:30). The code calculates
radiative equilibrium temperature solution,
thermal and PAH/vsg emission, scattering and polarization in
protostellar
geometries; good for computing spectral energy distributions
(SEDs),
polarization spectra, and images. The history of changes
are listed here.
Update, Please replace this subroutine in the src directory:
output.F90. Email me if you want to be alerted to new versions of
this or any other code: bwhitney (at) spacescience.org

3. HO-CHUNK.ttsre.2008,
the
previous version.
Latest update: Aug. 26, 2009. The history of changes
are listed here.
Note: we no longer supply a set of Kurucz and Nextgen atmosphere
models because they are available on the protostars
website.

4. HO-CHUNK.ttsscat.20090521,
calculates
scattering and polarization in
protostellar geometries (star surrounded by disk and/or envelope,
bipolar cavities, outflows); good for computing
optical/near-IR images where most of the emitted radiation comes from
the
central star and then scatters in the disk+envelope. Latest
update: May 21, 2009. The history of changes are listed
here.

More general circumstellar codes:

3. HO-CHUNK.sphere.20040407,
calculates
scattering and polarization in circumstellar dust or
electrons illuminated by a central
source; good for computing optical/near-IR images.
It's currently set up to compute an ellipsoidal envelope
and/or a disk. The instructions explain how you can
modify the geometry. Note: this code will be replaced by "csscat"
within a few months. It will do the same thing, just will derive
from the
ttsscat program and will be easier to maintain. Anyway "sphere"
is misnomer since it does 2-D and 3-D geometries.

4. HO-CHUNK.csre.20050228,
calculates
radiative equilibrium temperature solution,
thermal emission, scattering and polarization in circumstellar
dust illuminated by a central
source; good for computing SEDs, polarization spectra and
thermal images. It's currently set up to compute an ellipsoidal
envelope
and/or a disk. The instructions explain how you can
modify the geometry. The history of changes
are listed here.

Learning tools:

Here is a link to a
review article I wrote on Monte Carlo radiative transfer.

5. sphere_1d.20040407.
this
does isotropic scattering in a sphere. You can vary the
radial density profile. this is almost too boring a code.
But it computes intensity moments vs radius which seems to excite some
people.

6. slab.20040407, this is a
plane-parallel code that computes isotropic scattering. It
computes intensity moments as a function of optical depth and emergent
intensity as a function of angle. If you want to learn monte
carlo, this might be the best starting point. It has the fewest
lines of code.

7. blob.20040407, this
computes scattering and polarization off a spherical distribution of
particles. can be used to compute scattering off a planet for
example. This is a good learning tool if you want to learn
how to do polarization (though if you want to see more clever coding,
ask Jon Bjorkman for his routines). (and I haven't tried to clean
up the code, sorry).

All of these programs come as a gzipped tar file (e.g.,
hochunk3d_20140131.tgz or HO-CHUNK.ttsscat.20090521.tar.gz).
Here's how to install the latest version of hochunk3d:
1. Download the file by clicking on the link above
2. in your preferred directory, type
tar -xzvf hochunk3d_20140131.tgz
or if your downloader unzipped it for you already
tar xvf hochunk3d_20140131.tar
3. cd hochunk3d_20140131
4. open the instructions.txt file to find out the rest

All the programs come with sample runs and plotting files
(using IDL). They've been tested most extensively using Linux and
MacOS
compilers: g77, ifort, and gfortran. In the past, they have run
with IBM XLF, Absoft, lf95,
and pgfortran compilers but I don't have them anymore. They
probably still work.